Outflows are ubiquitous at the peak epoch of star formation (z~1-3), and are likely to play an important role in shaping the growth and evolution of galaxies. Near-IR integral field spectroscopy is a powerful tool to investigate the physical properties of galactic winds at this epoch because it enables us to kinematically disentangle them from gravitational motions, and to map the launch sites, extent, and geometry of outflows. I will present results from our SINFONI and KMOS outflow studies at z~1-3, focusing on properties and scaling relations of SF-driven outflows resolved on ~1-2 kpc scales. We find that the outflow velocity and mass loading factor correlate with the local star formation surface density, but the mass loading factors are always low (<= 0.5). The vast majority of the outflowing material does not have sufficient velocity to escape from the galaxy halos, but will be re-accreted and contribute to the chemical enrichment of these galaxies. I will discuss these results in the context of our study of global outflow properties and demographics from the KMOS^3D survey (including AGN driven outflows).